As shown in [1]}, Sect. 4.6, the pipeline propagated variance of the datacube does not take into account the additional correlated noise due to the interpolation process. In DR1, we replaced the propagated variance of each individual datacube with a noise estimate derived from the datacube after masking the light sources, which is then rescaled to account for the impact of the correlated noise ([2]}, Sect. 3.5.1). The limitation is that this noise estimate is not valid for bright sources that are not sky-dominated. Another inaccuracy is that this noise estimate is by construction constant across the field of view and thus does not account for possible flat field variation. Thus, to address these limitations, we implemented a different scheme for MXDF: we computed the median ratio between the propagated variance and the variance estimated on the datacube itself after adjusting for correlated noise. This ratio has a slight evolution with the wavelength from 2.45 in the blue to 2.55 in the red. The propagated variance is then simply multiplied by this factor.
